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We investigate the dynamical evolution of star clusters during theirformation, assuming that they are born from a turbulent starless clump of agiven mass that is embedded within a parent self-gravitating molecular cloudcharacterized by a particular mass surface density. In contrast to the standardpractice of most $N$-body studies, we do not assume that all stars are formedat once. Rather, we explore the effects of different star formation rates onthe global structure and evolution of young embedded star clusters, alsoconsidering various primordial binary fractions and mass segregation levels.Our fiducial clumps studied in this paper have initial masses of $M_{\rm cl} =3000\,M_\odot$, are embedded in ambient cloud environments of $\Sigma_{\rmcloud} = 0.1$ and 1 g cm$^{-2}$, and gradually form stars with an overallefficiency of 50% until the gas is exhausted. We investigate star formationefficiencies per free-fall time in the range $\epsilon_{\rm ff}=0.01$ to 1, andalso compare to the instantaneous case ($\epsilon_{\rm ff}=\infty$) of Paper I.We show that most of the interesting dynamical processes that determine thefuture of the cluster, happen during the early formation phase. In particular,the ejected stellar population is sensitive to the duration of star clusterformation: for example, clusters with longer formation times produce morerunaway stars, since these clusters remain in a dense state for longer, thusfavouring occurrence of dynamical ejections. We also show that the presence ofradial age gradients in star clusters depends sensitively on the star formationefficiency per free fall time, with observed values being matched best by ourslowest forming clusters with $\epsilon_{\rm ff}\lesssim0.03$.

Star Cluster Formation from Turbulent Clumps. II. Gradual Star Cluster Formation